This material is based upon work
supported by the
National Science
Foundation under NSF-RUI Grant
No. AST-0307365, Michigan Space Grant Consortium, and the National Aeronautics
and Space Administration
Astrophysics Theory Program.

Our previous studies of
pulse profiles from radio pulsars have used a core with a single cone beam.
We propose an improved model, featuring a core with two cones coaxial to
the magnetic pole, to account for profiles with up to five components. We
follow recent results suggesting that the radius of the inner cone is independent
with frequency, while the outer cone has the standard radius-to-frequency
mapping. Fits of pulse profiles of radio pulsars with accurate parallax distances
allow us to estimate the total intrinsic luminosity of each beam component.
These fit parameters can be used to test the standard candle nature of radio
pulsars. In developing this new model, we have fit the best available five-peaked
profiles with the core-two-cone model, as well as the three-peaked profiles
previously fitted. We will include this model in our population statistics
simulation of
radio and g-ray pulsars within the context
of polar cap and outer gap emission models. Performing a new statistical study
of the number
of peaks
in the radio and g-ray profiles will aid in distinguishing
these
high-energy emission models and the location of the accelerator.